White dwarfs are well studied objects. The relative simplic-
ity of their physics allows to obtain very detailed models which can
be ultimately compared with their observed properties. Among them
there is a specific class of stars, the ZZ–Ceti stars that are character-
ized by the extreme stability of their periods of pulsation. The rate
of change of the period is closely related to the characteristic cooling
time of the star, which can be accurately computed. This property not
only allows to directly test the evolution of white dwarfs but also to
constrain parameters of any new physical theory able to perturb the
cooling regime. This technique has been successfuly aplied to the case
of axions and can be used to constrain the properties of other theoreti-
cal particles. The program we propose here consists in using the ability
of the Antartic plateau to perform long time and non–interrupted ob-
servations to establish the seismological properties of a well defined set
of variable white dwarfs (and other stable pulsators).